Table 2.
Significant spectral lines identified in the time-averaged Resolved+Xtend spectra.
| Line ID | Erest | vraw | vreal | σ | σraw | EW | Δ C-stat | MC significance |
|---|---|---|---|---|---|---|---|---|
| Unit | [keV] | [km s−1] | [km s−1] | [eV] | [km s−1] | [eV] | [%] | |
| Ni XXVII Hew | 7.806 | ![]() |
![]() |
0† | 0† | ![]() |
13 | 99.9 |
| Fast Fe XXVI Lyα1 | 6.973 |
|
−1290 ± 90 | < 3.2 | < 150 | ![]() |
12 | 99.2★ |
| Fast Fe XXVI Lyα2 | 6.952 | ![]() |
||||||
| Slow Fe XXVI Lyα1 | 6.973 |
|
|
6.2−2.0+13.8† | 270−90+590† | 52 ± 16 | 89 | > 99.9 |
| Slow Fe XXVI Lyα2 | 6.952 | ![]() |
||||||
| Fe XXV Hew | 6.700 |
|
|
|
|
![]() |
177 | > 99.9 |
| Fe XXV Hey | 6.668 | ![]() |
||||||
| Fe I Kα1 | 6.404 | 850+290−540 |
|
|
|
20 ± 10 | 18 | > 99.9 |
| Fe I Kα2 | 6.391 | 10 ± 5 | ||||||
| Cr XXIII Hew | 5.682 | 50 ± 80 | ![]() |
0† | 0† | ![]() |
11 | 99.5 |
| Ca XX Lyα | 4.105 | ![]() |
![]() |
|
![]() |
14 ± 8 | 15 | > 99.9 |
| S XVI Lyα | 2.622 | ![]() |
![]() |
|
![]() |
![]() |
20 | > 99.9 |
| Xtend Only | ||||||||
| Ne X Lyα | 1.022 | 0† | – | 0† | 0† | 40
|
67 | > 99.9 |
Notes. Errors and upper limits are computed at a 90% confidence level. † indicates parameters that were frozen during the fit or are at the limit of their allowable parameter space. The MC significance was computed from 1000 fakeit simulations of the lines to account for photon noise. ★ The MC computation on this line was computed on a broader velocity space account for the look elsewhere effect at high velocity shifts. See Sect. 3.1 for details of the MC computation. The quoted rest energies are adopted from NIST, with the energies of all unresolved H-like lines set at the 2/1 mean of the two main individual transitions. Common widths and blueshifts between different lines indicate complexes for which these values were linked during the fit. The norms of the individual components of the H-like complexes were tied with a ratio of 1−2 during the fit. vreal values include the total velocity correction of −117 ± 13 km s−1 derived for the observation. σraw values are converted directly from the measured σ, and thus include an artificial contribution of 28 km s−1 from the evolution of the orbital velocity of the BH within the observation. See Appendix A for the detailed computation of the corrections.
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